Photographic observations of the cloud in the neighbourhood of libration point L 5 of the Earth-Moon system

Winiarski, M.

doi:10.1007/bf00058142

Cited by 14 publications

(4 citation statements)

References 6 publications

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“…Smith et al 1982; Yoder et al 1983; Yoder, Synnott & Salo 1989). Another example of a Trojan configuration closer to home is provided by the extensive dust clouds in the neighbourhood of the L 5 point of the Earth–Moon system claimed by Winiarski (1989).…”

Section: Introductionmentioning

confidence: 99%

Asteroids in the inner Solar system - I. Existence

Tabachnik

Evans

2002

Monthly Notices of the Royal Astronomical Society

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Ensembles of in‐plane and inclined orbits in the vicinity of the Lagrange points of the terrestrial planets are integrated for up to 100 Myr. The integrations incorporate the gravitational effects of the Sun and the eight planets (Pluto is neglected). Mercury is the least promising planet, as it is unable to retain tadpole orbits over 100‐Myr time‐scales. Mercurian Trojans probably do not exist, although there is evidence for long‐lived, corotating horseshoe orbits with small inclinations. Both Venus and the Earth are much more promising, as they possess rich families of stable tadpole and horseshoe orbits. Our survey of Trojans in the orbital plane of Venus is undertaken for 25 Myr. Some 40 per cent of the survivors are on tadpole orbits. For the Earth, the integrations are pursued for 50 Myr. The stable zones in the orbital plane are larger for the Earth than for Venus, but fewer of the survivors (∼20 per cent) are tadpoles. Both Venus and the Earth also have regions in which inclined test particles can endure near the Lagrange points. For Venus, only test particles close to the orbital plane are stable. For the Earth, there are two bands of stability, one at low inclinations and one at moderate inclinations The inclined test particles that evade close encounters are primarily moving on tadpole orbits. Two Martian Trojans (5261 Eureka and 1998 VF31) have been discovered over the last decade and both have orbits moderately inclined to the ecliptic (203 and 313 respectively). Our survey of in‐plane test particles near the Martian Lagrange points shows no survivors after 60 Myr. Low‐inclination test particles do not persist, as their inclinations are quickly increased until the effects of a secular resonance with Jupiter cause destabilization. Numerical integrations of inclined test particles for time‐spans of 25 Myr show stable zones for inclinations between 14° and 40°. However, there is a strong linear resonance with Jupiter that destabilizes a narrow band of inclinations at ∼29°. Both 5261 Eureka and 1998 VF31 lie deep within the stable zones, which suggests that they may be of primordial origin.

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Section: Introductionmentioning

confidence: 99%

Asteroids in the inner Solar system - I. Existence

Tabachnik

Evans

2002

Monthly Notices of the Royal Astronomical Society

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“…Such a pioneer photographical documentation has been first performed by Kordylewski (1961). According to the other above-mentioned successful trials (Vanysek 1969;Roach 1975;Winiarski 1989), the KDC can be visually detected only from small phase angles (determined by the observer, the Sun and the L4/L5 point), i.e. at or near "full dust moon".…”

Section: Discussionmentioning

confidence: 99%

“…Analyzing the data from the Rutgers OSO-6 Zodiacal Light Analyzer experiment, Roach (1975) concluded that these dust clouds do exist in the L4 and L5 points, their angular size is about 6 o as seen from the Earth, and they move around the libration points. Using a number of parallel cameras at the observing station Roztoki Górne, Winiarski (1989) determined that the colours of the dust clouds near the L4 and L5 points differ from those of the counterglow (gegenschein), which means that the dust particles constituting them are also different.…”

Section: Discussionmentioning

confidence: 99%

Celestial mechanics and polarization optics of the Kordylewski dust cloud in the Earth–Moon Lagrange point L5 – Part II. Imaging polarimetric observation: new evidence for the existence of Kordylewski dust cloud

Slíz-Balogh

Barta

Horváth

2018

Monthly Notices of the Royal Astronomical Society

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Telescopes mounted with polarizers can study the neutral points of the Earths atmosphere, the solar corona, the surface of planets/moons of the Solar System, distant stars, galaxies and nebulae. These examples demonstrate well that polarimetry is a useful technique to gather astronomical information from spatially extended phenomena. There are two enigmatic celestial objects that can also effectively be studied with imaging polarimetry, namely the Kordylewski dust clouds (KDCs) positioned around the L4 and L5 triangular Lagrangian libration points of the Earth-Moon system. Although in 1961 the Polish astronomer, Kazimierz Kordylewski had observed two bright patches near the L5 point with photography, many astronomers assume that these dust clouds do not exist, because the gravitational perturbation of the Sun, solar wind and other planets may disrupt the stabilizing effect of the L4 and L5 Lagrange points of the Earth and Moon. Using ground-born imaging polarimetry, we present here new observational evidence for the existence of the KDC around the L5 point of the Earth-Moon system. Excluding artefacts induced by the telescope, cirrus clouds or condensation trails of airplanes, the only explanation remains the polarized scattering of sunlight on the particles collected around the L5 point. By our polarimetric detection of the KDC we think it is appropriate to reconsider the pioneering photometric observation of Kordylewski. Our polarimetric evidence is supported by the results of simulation of dust cloud formation in the L5 point of the Earth-Moon system presented in the first part of this paper.

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“…With the help of the Orbiting Solar 40 Observatory, Roach also detected the KDCs in 1975 [12]. In 1989, the clouds were again photographed by Winiarski [13]. On the other hand, many scholars are strongly skeptical about the existence of the KDCs (Roosen, Harrington & Jeffreys 1967; Bruman 1969; Valdes & Freitas 1983; Igenbergs et al 2012) [14].…”

Section: Current Observation Status Of the Kdcsmentioning

confidence: 99%

Ground- and Space-Based Observation of Kordylewski Clouds

et al. 2021

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The ghost dust clouds in the vicinity of Earth-Moon triangular libration points are known as the “Kordylewski clouds” (KDCs). Objects in the KDCs may give hints to the physical, chemical, and dynamical properties of the solar system. As a result, in situ exploration of the KDCs can help us understand the evolution of our solar system. This paper first summarizes the observation history of the KDCs. Based on the properties of the KDCs, a ground- and space-based observation concept is proposed, using the CAST 100 platform developed by DFH and ground stations. Some details of the concept are exploited.

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Photographic observations of the cloud in the neighbourhood of libration point L 5 of the Earth-Moon system

Cited by 14 publications

References 6 publications

Asteroids in the inner Solar system - I. Existence

Asteroids in the inner Solar system - I. Existence

Celestial mechanics and polarization optics of the Kordylewski dust cloud in the Earth–Moon Lagrange point L5 – Part II. Imaging polarimetric observation: new evidence for the existence of Kordylewski dust cloud

Ground- and Space-Based Observation of Kordylewski Clouds

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